Tuesday, 3 December 2019

First Maps of Uranus' Stratosphere

Dr. Mike Roman of @PhysicsUoL has published the first IR maps of Uranus' cold stratosphere using the @ESO VISIR instrument, showing warm 'caps' of hydrocarbon emission, and evidence of mid-latitude upwelling from the troposphere to the stratosphere.




The image contrasts troposphere (warm equator and poles, cool mid-latitudes) and stratosphere (warm poleward of ±30 degrees, cool equator), and has a bonus: first thermal-IR glimpses of #Uranus' rings at 18 ┬Ám (published with ALMA data in Molter et al., https://t.co/VzFp5XMb1K)

We combined Mike's VISIR thermal maps with a seasonal photochemistry model from Julie Moses (https://t.co/7nnY4vDM8P) to predict what #Uranus would have looked like if we'd had a VLT for decades... here's a GIF spanning 1966-2050 in two wavelengths.


But this is *only* two wavelengths - with the @NASAWebb MIRI instrument we hope to get full spectral and spatial maps of Uranus' cold stratosphere to understand how/why its chemistry/circulation differs to other worlds, so for us #WebbIsWorthTheWait

Monday, 25 November 2019

Why Study Planetary Atmospheres?

How does looking at weather on other worlds help inform our understanding of the Earth’s atmosphere?

Think of all the planets in our solar system as offering a continuum of different outcomes for atmospheric evolution, based primarily on the soup of species that were initially accreted by the protoplanet, the distance of the planet from the Sun today, and the dynamical properties of the planet (e.g., its size and rate of rotation, which determine the banded pattern of winds).  By comparing how atmospheric meteorology, chemistry, clouds and dynamics differ from one world to the next, we get a better understanding of the physical and chemical rulebook that governs what an atmosphere (or a climate) will actually be like.  Science is all about experimentation – tweaking one parameter and seeing how a system changes.  We can’t do that sort of mass experimentation on our home world (well, ahem, ignoring the massive amount of CO2 we’re pumping into our fragile atmosphere), but the planets of our solar system (and indeed, exoplanets) offer a ready-made experiment, out there for us to explore.  If we find that a theory of atmospheres based on Earth doesn’t work for Mars, or for Saturn, then we need to know why it doesn’t work – and that might mean tweaking the theory.

Now, that all might sound straightforward, and ultimately is the direction planetary atmospheric scientists might want to head.  But for now, we know that the conditions are so different from world to world that it’s hard to determine whether our universal theories are inaccurate, or whether the data are simply incomplete or misleading.  For example, Saturn has no solid boundaries (mountains, continents, valleys) to get in the way of perfect fluid dynamical flows, so it’s a very different regime from Earth.  Furthermore, its clouds and precipitation exist in a hydrogen rich atmosphere (the lightest gas in the universe), which is totally different to the Earth’s nitrogen-oxygen atmosphere.  So today, I’d say we’re at the stage (with missions like Cassini and Juno) of trying to properly measure and observe these unusual atmospheres.  The next step is to confirm that we can recreate them numerically as a simulation (in just the same way as a terrestrial weather and climate model works).

How can other planets give us a glimpse of our future?

A lot of what I said above also applies here – our planet exists of a continuum of planetary types, showing how worlds can end up in different states depending on small changes at the start of their evolution.  Take Venus, Earth, and Mars, for example:  these worlds might all have started off under conditions that weren’t so very different, but over the aeons those differences were amplified – Venus becoming the hellish world of high temperatures and corrosive atmosphere; Mars freezing to become a barren desert.  These are great examples of divergent evolution from shared origins.  Now, we humans have been doing an uncontrolled experiment with our own fragile atmosphere since the industrial revolution, vastly upsetting the balance of molecules in our atmosphere and leading to today’s climate emergency.  Venus stands as a stark warning of what happens to worlds with too much carbon dioxide.  Mercifully, we know that this is avoidable, if we only had the willpower to change our ways.

Wednesday, 26 June 2019

All About Space: Why Explore the Ice Giants?

In June 2019 I was asked to provide an entry for All About Space magazine's "Ask Space" section, with the following topic:

All About Space Spring 2019

Why is it important to study the ice giants, Uranus and Neptune?
Dr. Leigh Fletcher
Associate Professor in Planetary Science, University of Leicester

Uranus and Neptune have never had a dedicated spacecraft mission, having been visited only once by the brief flyby mission of Voyager 2, three decades ago.  These distant Ice Giants are the least-explored type of planet in our Solar System, intermediate between the big hydrogen-rich Gas Giants (Jupiter and Saturn) and the smaller rocky planets.  And yet Neptune-sized worlds appear to be commonplace in our galaxy, a natural outcome of the chaotic process of planet formation.  A mission to these icy worlds is the logical next step in humanity’s exploration of our planetary system, to understand how Uranus and Neptune formed, to explore their deep water-rich interiors and exotic hot ices, their stormy atmospheres, and their complex magnetic fields that are totally unlike anything witnessed at Jupiter and Saturn.  The two worlds are superb examples of how planets with shared origins can go down different evolutionary paths:  Neptune as the archetype for Ice Giants, with its seasonal tilt and powerful winds; Uranus as the oddball, with its extreme tilted inclination and sluggish atmosphere.  And both worlds harbour diverse satellite systems, from Uranus’ collection of natural icy satellites with evidence of extreme geological activity, to Neptune’s captured satellite Triton, a visitor from the more distant Kuiper Belt, which may harbour a sub-surface ocean and exhibits erupting geysers from its surface.  For all these reasons and more, scientists across the globe are urging their space agencies to mount an ambitious robotic mission to explore these worlds in the coming decade.

Thursday, 20 June 2019

First Thermal Detection of the Rings of Uranus

The image above is a composite image of Uranus’s atmosphere and rings at radio wavelengths, taken with the ALMA array in December 2017. The image shows thermal emission, or heat, from the rings of Uranus for the first time, enabling scientists to determine their temperature: a frigid 77 Kelvin (-320 F). Dark bands in Uranus’s atmosphere at these wavelengths show the presence of molecules that absorb radio waves, in particular hydrogen sulfide gas. Bright regions like the north polar spot (yellow spot at right, because Uranus is tipped on its side) contain very few of these molecules. (UC Berkeley image by Edward Molter and Imke de Pater)

The rings of Uranus are invisible to all but the largest telescopes — they weren’t even discovered until 1977 — but they’re surprisingly bright in new heat images of the planet taken by two large telescopes in the high deserts of Chile.

The thermal glow gives astronomers another window onto the rings, which have been seen only because they reflect a little light in the visible, or optical, range and in the near-infrared. The new images taken by the Atacama Large Millimeter/submillimeter Array (ALMA) and the Very Large Telescope (VLT) allowed the team for the first time to measure the temperature of the rings: a cool 77 Kelvin, or 77 degrees above absolute zero — the boiling temperature of liquid nitrogen and equivalent to 320 degrees below zero Fahrenheit.

The observations also confirm that Uranus’s brightest and densest ring, called the epsilon ring, differs from the other known ring systems within our solar system, in particular the spectacularly beautiful rings of Saturn.

“Saturn’s mainly icy rings are broad, bright and have a range of particle sizes, from micron-sized dust in the innermost D ring, to tens of meters in size in the main rings,” said Imke de Pater, a UC Berkeley professor of astronomy. “The small end is missing in the main rings of Uranus; the brightest ring, epsilon, is composed of golf ball-sized and larger rocks.”

By comparison, Jupiter’s rings contain mostly small, micron-sized particles (a micron is a thousandth of a millimeter). Neptune’s rings are also mostly dust, and even Uranus has broad sheets of dust between its narrow main rings.

“We already know that the epsilon ring is a bit weird, because we don’t see the smaller stuff,” said graduate student Edward Molter. “Something has been sweeping the smaller stuff out, or it’s all glomming together. We just don’t know. This is a step toward understanding their composition and whether all of the rings came from the same source material, or are different for each ring.”

Rings could be former asteroids captured by the planet’s gravity, remnants of moons that crashed into one another and shattered, the remains of moons torn apart when they got too close to Uranus, or debris remaining from the time of formation 4.5 billion years ago.

detail of Uranian rings
Uranian rings:  Near-infrared image of the Uranian ring system taken with the adaptive optics system on the 10-meter Keck telescope in Hawaii in July 2004. The image shows reflected sunlight. In between the main rings, which are composed of centimeter-sized or larger particles, sheets of dust can be seen. The epsilon ring seen in new thermal images is at the bottom. (UC Berkeley image by Imke de Pater, Seran Gibbard and Heidi Hammel, 2006)

The new data were published this week in The Astronomical Journal. De Pater and Molter led the ALMA observations, while Michael Roman and Leigh Fletcher from the University of Leicester in the United Kingdom led the VLT observations.

“The rings of Uranus are compositionally different from Saturn’s main ring, in the sense that in optical and infrared, the albedo is much lower: they are really dark, like charcoal,” Molter said. “They are also extremely narrow compared to the rings of Saturn. The widest, the epsilon ring, varies from 20 to 100 kilometers wide, whereas Saturn’s are 100’s or tens of thousands of kilometers wide.”

The lack of dust-sized particles in Uranus’s main rings was first noted when Voyager 2 flew by the planet in 1986 and photographed them. The spacecraft was unable to measure the temperature of the rings, however.

To date, astronomers have counted a total of 13 rings around the planet, with some bands of dust between the rings. The rings differ in other ways from those of Saturn.

“It’s cool that we can even do this with the instruments we have,” he said. “I was just trying to image the planet as best I could and I saw the rings. It was amazing.”

Both the VLT and ALMA observations were designed to explore the temperature structure of Uranus’ atmosphere, with VLT probing shorter wavelengths than ALMA.

“We were astonished to see the rings jump out clearly when we reduced the data for the first time,” Fletcher said.

What's amazing about this is that the Uranus observations were targeting the thermal structure of the atmosphere.  When I first processed the data, I was astonished to see the rings.  That's never happened before.  I actually thought I'd messed up and created artefacts in the mid-IR imaging... (heh, wouldn't be the first time). It was only when I zoomed out that I realised what I was seeing.  The Uranus thermal data was not supposed to be taken... the panel rejected us. But our Jupiter programme was getting harder and harder to finish (it was sinking lower in the sky), so they offered to let me change target and.... hey-presto... discovery! 

This presents an exciting opportunity for the upcoming James Webb Space Telescope, which will be able provide vastly improved spectroscopic constraints on the Uranian rings in the coming decade.

Images of the Uranian ring system captured at different wavelengths by the ALMA and VLT telescopes. The planet itself is masked since it is very bright compared to the rings. (Images by Edward Molter, Imke de Pater, Michael Roman and Leigh Fletcher, 2019)


The Berkeley research was funded by the National Aeronautics and Space Administration (NNX16AK14G). Work at the University of Leicester was supported by the European Research Council (GIANTCLIMES) under the European Union’s Horizon 2020 research and innovation program (723890)..

Wednesday, 19 June 2019

NASA's Webb Telescope Will Survey Saturn and its Moon Titan

This image shows a giant Saturnian storm that was observed at mid-infrared wavelengths in 2011.
This image shows a giant Saturnian storm that was observed at mid-infrared wavelengths by the European Southern Observatory’s Very Large Telescope in 2011. The warm gases powering the storm make it glow brightly compared to the rest of the planet.
Credits: L. Fletcher (University of Leicester) and ESO

Christine Pullen writes about our plans to use the James Webb Space Telescope to explore Saturn's atmospheres, rings, and satellites, continuing the legacy of the Cassini mission:
If you stop a random person on the sidewalk and ask them what their favorite planet is, chances are their answer will be Saturn. Saturn’s stunning rings are a memorable sight in any backyard telescope. But there is still a lot to learn about Saturn, especially about the planet’s unique weather and chemistry, as well as the origin of its opulent ring system. After its launch in 2021, NASA’s James Webb Space Telescope will observe Saturn, its rings, and family of moons as part of a comprehensive solar system program.
This study will be conducted through a Guaranteed Time Observations program headed up by Heidi Hammel, a planetary astronomer and executive vice president of the Association of Universities for Research in Astronomy (AURA) in Washington, D.C. Hammel was selected by NASA as a Webb Interdisciplinary Scientist in 2002.
“The purpose of this program is to demonstrate the capabilities of Webb for solar system observations, including observing bright objects, tracking moving objects, and spotting faint targets next to bright ones,” Hammel explained. “The data will be made available to the solar system community as soon as possible to show them that Webb can do what we’ve promised them.”
Webb will pick up where NASA’s Cassini spacecraft left off. Cassini orbited Saturn for 13 years, from 2004 until the mission ended in 2017 when the spacecraft plunged into Saturn’s atmosphere. Since then, programs like the Hubble Space Telescope’s Outer Planet Atmospheres Legacy program and ground-based measurements have been the only way to monitor Saturn.

Saturn experiences auroras, also known as northern and southern lights, just like Earth.
Saturn experiences auroras, also known as northern and southern lights, just like Earth. Here, Hubble ultraviolet-light observations of an aurora are superposed on a visible-light image of the planet.
Credits: NASA, ESA, J. Clarke (Boston University), and Z. Levay (STScI)
Saturn’s Seasons
Saturn is tilted on its axis just like the Earth, and as a result, it also experiences seasons as it orbits the Sun. However, since the Saturnian year is 30 Earth-years long, each season lasts about 7-1/2 years. Cassini arrived during the southern hemisphere’s summer (winter in the northern hemisphere). Now it is summer in the northern hemisphere. Astronomers are eager to look for seasonal changes in Saturn’s atmosphere.
“These observations will give us a full assay of the Saturnian system to see what’s changed, to see how the seasons have evolved since Cassini’s last glimpses and to harness capabilities Webb has that Cassini never did,” said Leigh Fletcher of the University of Leicester, England, a principal investigator on the program.
In late 2010, a monster storm erupted in Saturn’s northern hemisphere. It began as a tiny spot but grew rapidly, until by the end of January 2011 it encircled the planet. Astronomers were surprised because such storms normally don’t form until after the summer solstice, which occurred in 2017. They will be watching for more storms as Saturn’s northern hemisphere moves from summer into fall over the course of Webb’s mission.
Storms aren’t the only atmospheric phenomena that Saturn and Earth share. Saturn also experiences auroras, or northern and southern lights. Those auroras trigger chemical changes in Saturn’s atmosphere, breaking apart some molecules and allowing new ones to form. Webb will look for signatures of that unusual chemistry glowing at mid-infrared wavelengths, particularly in the north polar region.

Hazy layers of hydrocarbons enshroud Saturn’s moon, Titan. On its surface, methane rivers flow into tar-edged seas.
Hazy layers of hydrocarbons enshroud Saturn’s moon, Titan. On its surface, methane rivers flow into tar-edged seas.
Credits: NASA/JPL-Caltech/Space Science Institute
Titan, Saturn’s Largest Moon
Saturn’s largest moon, Titan, also will fall under Webb’s powerful gaze. Titan is unique because it is the only moon in our solar system with a substantial atmosphere. In fact, it’s bigger than the planet Mercury. The atmospheric pressure on Titan is about 50% greater than on Earth. Like Earth, that atmosphere is mostly nitrogen, but Titan also has vaporous hydrocarbons like methane. Titan also is much colder than Earth, with a surface temperature around minus 290° Fahrenheit (minus 180° Celsius).
Within Titan’s atmosphere, chemical reactions are constantly churning its composition. Molecules are broken up into their constituents like carbon, hydrogen, oxygen and nitrogen. Those atoms form new molecules, which percolate through the air and settle at whichever pole is currently experiencing winter.
“Titan’s atmosphere is like a big chemistry lab,” said Conor Nixon of NASA’s Goddard Space Flight Center, Greenbelt, Maryland., a principal investigator on the program. Nixon and his colleagues will use Webb’s Near-Infrared Spectrograph (NIRSpec) and Mid Infrared Imager (MIRI) to study these molecules in much greater detail than Cassini’s instruments allowed.
Titan also is the only object in our solar system besides Earth with liquid seas and lakes on its surface. While Earth has a water cycle in which water evaporates, falls as rain, and flows down rivers to the ocean, Titan experiences a similar cycle with methane. On Titan, methane rain carves river beds through rock-hard water ice before flowing into tar-edged seas. Cassini and its Huygens probe from the European Space Agency, which landed on Titan in 2004, made remarkable discoveries about this Saturnian moon. Webb will study Titan’s seasonal climate cycles to compare them to astronomers’ models.
“Titan has clouds and weather that we can see changing in real time. Its chemistry is very different from Earth’s, but it’s still organic, carbon-based chemistry,” said Stefanie Milam of NASA Goddard, a co-investigator on the program.

Jupiter’s moons Io and Europa, and Saturn’s moons Enceladus and Titan, show remarkable geological activity for their small size.
Jupiter’s moons Io and Europa, and Saturn’s moons Enceladus and Titan, show remarkable geological activity for their small size, with features ranging from volcanoes and water plumes to possible subsurface oceans.
Credits: J Olmsted (STScI)
While Webb’s mission lifetime after launch is designed to be at least 5-1/2 years, it could potentially last 10 years or more. As a result, it could watch Saturn go from northern summer through the autumnal equinox and back to southern spring. That would nearly “complete the circle” begun when Cassini arrived during southern summer.
“We will genuinely have covered an entire Saturnian year. That would be quite an eye-opening experience,” said Fletcher.
The James Webb Space Telescope will be the world's premier space science observatory when it launches in 2021. Webb will solve mysteries in our solar system, look beyond to distant worlds around other stars, and probe the mysterious structures and origins of our universe and our place in it. Webb is an international project led by NASA with its partners, ESA (European Space Agency) and the Canadian Space Agency.
For more information about Webb, visit www.nasa.gov/webb.
By Christine Pulliam
Space Telescope Science Institute, Baltimore, Md.

Thursday, 3 January 2019

Tips for Student Presentations

[Health warning: personal preferences may differ between researchers!]

One of the key skills being developed in an undergraduate or graduate degree is the ability to communicate complex ideas in a succinct and accessible way.  This is tested several times during the Physics degree course here at Leicester, and common mistakes can lead to lost marks.  Here's a list of my own personal preferences for presentations, in case they're of use to the wider community.

  • Three Ts:  Tell them what you’re going to tell them; tell them; then tell them what you’ve told them.  Repetition of key points helps to reinforce them.  You’re telling a story, so make sure there are points in your slides to introduce, review, and summarise.
  • Show some enthusiasm:  If you don't, who else will?  I still get nervous before talks, but I try to channel this nervous energy into the talk, and I think it works.  Remember you're telling a story, and that even an audience of physicists would like to be entertained.  I'm not talking about becoming a stand-up comedian, but varying your voice and engaging your audience will all help you to be memorable.
  • Balance text and figures:  The audience will always be drawn towards your graphics, so these should dominate the slide with only bullet-points of text for key points.  Simple animations (e.g., building up a complex graphic with multiple slides) can often be really helpful.
  • Central Theme:  Use the first or second slide to define a central question or thesis that your presentation will address, and keep referring back to this in each Section and in the Conclusion.  That way, the reader will understand how each particular section fits into the wider presentation.
  • Numbered Sections and Footers:  Use numbered sections and subsections, as you would in a report, and make sure these numbers are prominent in slide headings/footers.  That way the audience knows where you are in the presentation, even if (ahem) they've just had 40 winks...  Also, use slide numbers with a [1/N] format, so the audience knows how long they need to sustain their attention...
  • Active Titles:  Use the slide title to drive home a message - this could be phrased as a question that you answer as you describe the slide; or it could be the key conclusion of that particular slide.  It helps the audience understand what you're trying to say.
  • Summarise sections:  At the end of a section, before moving on, try to include a few sentences/statements to say where we are in the presentation – what is the take-home message of the previous section, and what are we going to look at next?  This helps to avoid abrupt transitions between sections.
  • Referencing:  Figures and ideas should have references to the source (Author et al., yyyy) or a web URL - often DOIs (digital object identifiers) are helpful here.  You can include a slide with your references if the document is going to be read by people later on, but NEVER EVER end on this slide.
  • Keep to the point:  Don’t be tempted to go off topic or to introduce information that isn’t relevant to the central theme of the project – this can just lead to confusion and dilutes your take-home messages, and can mean that you run over your allotted time.
  • Practise makes perfect:  Time keeping is an essential skill - too short and you leave the audience wondering whether you're really cut out for presenting, too long and you offend the people coming after you.  And you really do want to leave time for questions at the end.  Practise out loud, preferably with an audience to give you some friendly critiques.
  • End on your Summary/Conclusions:  Don't ever fall into the trap of having the last slide say "Any Questions", or "Thanks", or "References".  Your last slide should contain a bulleted list of conclusions as a summary of what you've told them (preferably with an eye-catching graphic).  This should stay on the screen behind you as you answer questions.  
  • Don't be tempted to use fancy slide transitions:  Fade in and fade out is fine, but if I see the slide scrunch into a ball and bounce away, it's just distracting....

Oh, and Emily Lakdawalla at the Planetary Society has an excellent guide to conference presentations here:  http://www.planetary.org/blogs/emily-lakdawalla/2018/0206-speak-your-science.html